Download ppt - WISH

WISH Canada
- Canadian Science Interests Marcin Sawicki
with contributions from
Michael Balogh
Pauline Barmby
Scott Chapman
Jon Willis
Howard Yee
Canadian context
CCAT
~150 PhD-level
astronomers
JWST
ALMA
TMT
CFHT
Gemini (x2) JCMT ngCFHT
JWST: complement to
WISH
JWST: high-z galaxy hunter
NIRCAM
NIRSPEC
NIRISS
but small FOV => v. faint, more
numerous sources
TFI/NIRISS: built by ComDev Ottawa for CSA,
delivered to GSFC (summer 2013) for testing & integration
WISH Flip-type Wide-field Filter Exchange System
Current concept
from the WISH
study team
Toru’s WISH:
Canadians WISH for
+ luminous First Light sources (of course!)
+ Dark Energy (CFHTLS heritage)
...but also...
+ galaxy evolution out to z~5
+ galaxy clusters out to z~2
+ stellar populations in nearby galaxies
+ Solar System objects
WISH Canada
Ferrarese
Willott
Davidge
Kavelaars
McConnachie
Willis
Ellison
Pritchet
Scott
Doyon
Abraham
Webb
Yee
Sawicki
Barmby
Parker
Balogh
Chapman
Solar system objects
(see JJ Kavelaars’s talk on Tuesday)
WISH for Galactic star clusters
• metal-rich bulge globulars
• young massive clusters
• mass loss on the AGB and
RGB
Omega Cen: 30 arcmin Spitzer IRAC/MIPS (Boyer)
WISH for nearby galaxies
• Individual mass-losing
stars
• Integrated stellar mass
profiles
• Extinction law
• Rare, short-lived
evolutionary phases (eg
TP-AGB)
M33: 2MASS J-band (Jarrett) with WISH FOV
Why do we want to find
high-z galaxy clusters?
1. Growth of structures: the measurement
of cosmological parameters.
- independent of the geometric methods
such as SNe distance, CMB, BAO
- One of the very few ways to test GR at
very large scale.
2. Galaxy evolution, cluster formation:
effects of environment, large scale structure
These scientific goals require:
large samples and high redshift
Finding high-z clusters:
Cluster survey methods:
cost:
10$-$$
1. Optical/IR
$$ (rich clusters)
10
2. Sunyeav-Zeldovich effect
$$$
10
3. X-ray
(4. Weak gravitational lensing 10$$$) (limited to z<~0.8)
For finding relatively low-mass clusters at high-z,
multi-band opt/IR imaging proves to be the
most efficient.
The SBS (Stellar Bump Sequence) Method:
Muzzin, Wilson, Demarco, Lidman, Nantais, Hoekstra,
Yee & Rettura, 2013, ApJ, 767; arXiv:1301.5905)
The 1.6um peak
(produced by the minimum
in H-- opacity in spectra of
cool stars was first tested
as a feature useful for
photo-z by Sawicki (2002,
AJ)
The [3.6μm-4.5μm] color
forms an increasingly red
(observed) color
sequence from the 1.6μm
feature between z~0.8
and 1.7
SpARCS 163435+402151`
zphot = 1.25
VLT FORS2 spectroscopy
(2 masks, 3.75hrs integration each);
56 high-confidence redshifts,
12 (members) with 1.62<z<1.64
IRAC 3.6
z-band
A multi-wavelength view of distant,
massive
galaxy
clusters
• Current surveys of massive galaxy clusters extend to z=2
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Driven by optical-IR, X-ray or SZ observations over ~100 deg2
Surface density is of order 2 deg-2 (e.g. 1014 Msolar at z>0.8)
WISH wide and deep surveys will generate competitive samples
However, exploiting overlap with X-ray and SZ surveys enable key
science:
z > 1.5 represents a key period where such structures are collapsing
and attaining virial equilibrium
optical-IR searches + photo-z will detect clusters - but a lot of
filaments, LSS and projections as well
X-ray plus SZ turns this into an opportunity: we can identify virial and
non-virial structures and follow the impact of virialisation on baryons
Important baryon physics: BCG growth, central activity and satellite
quenching are imprinted upon the galaxy stellar populations and hot
gas
Science highlights: a zphot=1.9
X-ray (white), SZ (cyan), photoz selected galaxies (green)
High stellar mass
Low gas mass
Collapsing structures?
Distant (z>0.8) clusters on the X-ray vs IRAC luminosity plane:
X-ray selected (blue squares), IRAC selected + X-ray detected
(black squares), IRAC selected + X-ray faint (red upper limits).
Galaxy Evolution at 1<z<3
• Current surveys barely “resolve” the
peak in galaxy formation efficiency at
1<z<3
• Evolution of galaxies with M<1010 is
largely unconstrained.
Environment:
• At low redshift, the influence of
environment is most apparent in lowmass galaxies. It is largely unknown
what happens at z>1, where dynamical
times are much shorter, galaxies are
more gas-rich, etc.
Muzzin et al. (2013)
Morphology and Black Holes:
• AGN activity peaks at 1<z<3. Is this
associated with bulge growth?
Behroozi et al. (2013)
WISH and the 1<z<3 Universe
• WISH will allow stellar mass measurements of
quiescent galaxies with M>109, and star-forming
galaxies with M>108.
–Requires deep optical imaging as well. HSC and LSST
deep fields would match well.
–Morphologies of somewhat brighter galaxies will
enable tracking the mass growth of bulges and disks.
• Identification and characterization of low-mass
galaxies will provide great targets for follow-up with
TMT, ALMA
WISH and environment
• eROSITA will find a few hundred clusters at 1<z<1.5, and
a handful at higher redshift. Targeting these would be
very valuable.
• Other methods for identifying high-z protoclusters (e.g.
using massive radio galaxies) will provide a handful of
targets.
• Photometric selection may be possible, though lack of a
prominent red sequence may be a hindrance.
• These ideas should be developed more: low-mass
galaxies in protocluster environments would be very
interesting.
WISH and the z~4-5 Universe
Muzzin et al. (2013)
Ilbert et al. (2013)
Quiescent galaxies at z~5:
• Universe only 1.2Gyr old at z=5
• z=5 quiescent galaxies are fossils of z=10+ SF’ing
galaxies
10
sun
• observable to M~10 M with WISH (W5=26AB)
• ~1-100/sq deg/mag ?? Need ~100 sq deg
classic BzK
Daddi et al 2004
BzK @ z=2
WISH @ z=5
WISH and the z~4-5 Universe
“BzK” at z=4~5:
E(B-V)=0.6
E(B-V)=0.3
E(B-V)=0
Note: W0=28AB means we need
W5=26AB
For high-z quiescents,
shallower but wider
W5 would be better:
100 deg2 to W5=26
AB
For z=4-5 quiescents,
red filters (W5, W4)
are essential. They
can be 2 mags
shallower than bluer
filters.
WISH and CCAT
High Redshift Galaxy Evolution with CCAT
(Scott Chapman, on behalf of CCAT team)
12/01/13
• The integrated star
formation:
– Rises at z>3
– Peaks at z~1-3
– Declines at z<1
Log Density of Star Formation
WISH and CCAT
log(Redshift)
Hopkins et al. 2007
25
WISH and CCAT
• The majority of dust
appears to form at
3<z<6
• We currently have
few constraints on
how it forms
• We need CCAT to
measure it
26
WISH and CCAT
• CCAT will survey
>100 deg2 at
350, 450, 850um
• Designed for large
surveys and large
statistical samples
ALMA = Keck/TMT
CCAT =
WISH/LSST/DES/SDSS
• WISH will sample
around 4000A at z~5,
=> measure stellar
masses etc. of these
objects
WISH
4000A
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In summary
Strong interest in Canada spanning a range
of science
WISH highly complementary to other
Canadian projects (JWST, TMT, ngCFHT,
CCAT)
Capability and interest in Canada to work on
the Filter Exchange Unit (ComDev, UdeM)
Canadian Space Agency does not have a
regular proposal framework, so we are
working on them to secure support for
WISH-Canada